Context. The formation and evolution of ultra-short-period (USP) rocky planets is poorly understood. However, it is widely thought that these planets could not have formed at their present-day close-in orbits, but instead migrated inwards through interactions with outer neighbours. Aims. We aim to confirm and characterise the USP Earth-sized

We present a detailed optical and near-IR (NIR) spectral analysis of J-138717, a post-starburst galaxy at z = 1.8845 observed with JWST/NIRSpec, for which we derive a stellar mass of 3.5±0.2×10 10 M ⊙ and a stellar velocity dispersion of 198±10 km s ‑1. We estimate an age of ∼0.9 Gyr and a subsolar metallicity (between ‑0.4 and ‑0.2 dex). We find

We present the validation of TOI-2407 b, a warm Neptune-sized planet with a radius of $4.26\pm 0.26$ R $_{\oplus }$, orbiting an early M-type star with a period of 2.7 d and an equilibrium temperature of $705\pm 12$ K. The planet was identified by Transiting Exoplanet Survey Satellite (TESS) photometry and validated in this work through

We describe our approach to solving the problem of ensuring the solenoidality of the magnetic field vector in 3D inversions, as well as the estimation of the uncertainty in the inferred magnetic field. The solenoidality of the magnetic field vector is often disregarded in the inversion of spectropolarimetric data due to limitations in the

Using high-precision photometry, NASA's TESS space mission has discovered many intriguing transiting planet candidates. These discoveries require ground-based follow-up observations, including high-precision Doppler spectroscopy, to rule out false positive scenarios and measure the mass of the transiting planets. In this study, we present an

Context. Sunspots survive on the solar surface for timescales ranging from days to months. This requires them to be in an equilibrium involving magnetic fields and hydrodynamic forces. Unfortunately, theoretical models of sunspot equilibrium are very simplified as they assume that spots are static and possess a self-similar and axially symmetric